Detection of Circumstellar Material in a Normal Type Ia Supernova

Patat, F.; Chandra, Poonam; Chevalier, Roger A.; Justham, Stephen; Podsiadlowski, Ph.; Wolf, Christian; Gal‐Yam, A.; Pasquini, L.; Crawford, Ian; Mazzali, P. A.; Pauldrach, A. W. A.; Nomoto, Ken’ichi; Benetti, S.; Cappellaro, E.; Elias‐Rosa, N.; Hillebrandt, W.; Leonard, Douglas C.; Pastorello, A.; Renzini, A.; Sabbadin, F.; Simon, Joshua D.; Turatto, M.

doi:10.1126/science.1143005

Cited by 349 publications

(488 citation statements)

References 21 publications

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“…Comparing all these values to theoretical predictions on properties of the CSM from different progenitor scenarios of SNe Ia, a value of M CSM 0.8 M ⊙ at a distance of about 10 16 cm is larger than what most SD and DD scenarios predict (Patat et al 2007;Sternberg et al 2011;Chomiuk et al 2012;Raskin & Kasen 2013;Shen, Guillochon & Foley 2013;Soker et al 2013;Ruiter et al 2013;Margutti et al 2014). This seems to indicate that the CSMinteraction as an origin of the observed early UV excess of SN 2012cg is quite unlikely.…”

Section: Cooling Of Shock-heated Csmmentioning

confidence: 71%

“…In the SD scenario, CSM is generally expected to be present around the progenitor due to pre-explosion mass loss in a binary system (Patat et al 2007;Sternberg et al 2011;Dilday et al 2012). Also, some recent studies have suggested that a significant mass of CSM might be formed in the DD scenario:…”

Section: Cooling Of Shock-heated Csmmentioning

confidence: 99%

“…On the one hand, some narrow absorption signatures of circumstellar material (CSM) have been detected in some SNe Ia (Patat et al 2007;Sternberg et al 2011;Dilday et al 2012). This has been suggested to be evidence that supports the SD scenario because such CSM is generally expected to exist around SN Ia progenitor as the result of mass transfer from the companion star, as well as from WD winds.…”

Section: Introductionmentioning

confidence: 99%

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Constraining the progenitor of the Type Ia Supernova SN 2012cg

Liu

Stancliffe

2016

Mon. Not. R. Astron. Soc.

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The nature of the progenitors of Type Ia supernovae (SNe Ia) is not yet fully understood. In the single-degenerate (SD) scenario, the collision of the SN ejecta with its companion star is expected to produce detectable ultraviolet (UV) emission in the first few days after the SN explosion within certain viewing angles. It was recently found that the B − V colour of the nearby SN Ia SN 2012cg at about sixteen days before the maximum B-band brightness was about 0.2 mag bluer than those of other normal SNe Ia, which was reported as the first evidence for excess blue light from the interaction of normal SN Ia ejecta with its companion star. In this work, we compare current observations for SN 2012cg from its pre-explosion phase to the late-time nebular phase with theoretical predictions from binary evolution and population synthesis calculations for a variety of popular progenitor scenarios. We find that a main-sequence donor or a carbon-oxygen white dwarf donor binary system is more likely to be the progenitor of SN 2012cg. However, both scenarios also predict properties which are in contradiction to the observed features of this system. Taking both theoretical and observational uncertainties into account, we suggest that it might be too early to conclude that SN 2012cg was produced from an explosion of a Chandrasekhar-mass white dwarf in the SD scenario. Future observations and improved detailed theoretical modelling are still required to place a more stringent constraint on the progenitor of SN 2012cg.

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Section: Cooling Of Shock-heated Csmmentioning

confidence: 71%

Section: Cooling Of Shock-heated Csmmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Constraining the progenitor of the Type Ia Supernova SN 2012cg

Liu

Stancliffe

2016

Mon. Not. R. Astron. Soc.

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“…However, there are a few SNe Ia that show strong evidence for the SD channel, possibly with a red giant (RG) companion. Photoionization and subsequent recombination of circumstellar medium (CSM) has been observed in relatively normal SNe Ia (Patat et al 2007;Blondin et al 2009;Simon et al 2009), and CSM has been detected in the spectra of at least 20% of SNe Ia in spiral galaxies (Sternberg et al 2011) and has been linked to SN Ia explosion properties (Foley et al 2012b).…”

Section: Introductionmentioning

confidence: 99%

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Silverman¹,

Nugent

Gal‐Yam

et al. 2015

Proc. IAU

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Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the beststudied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogenrich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by Hα emission (with widths of ∼2000 km s −1 ) and exhibit large Hα/Hβ intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He i emission. They also show possible evidence of dust formation through a decrease in the red wing of Hα 75-100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na i D absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be −21.3 mag M R −19 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date.

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“…Recently, there has been a revived effort to identify additional signatures, such as the contribution to the early-time light curve from a possible companion (e.g. Kasen 2010;Bloom et al 2012;Brown et al 2012), Na I D line absorption features interpreted as evidence for circumstellar material (Patat et al 2007;Sternberg et al 2011;Dilday et al 2012), gamma-ray line and continuum emission (e.g. Sim & Mazzali 2008;Maeda et al 2012;Summa et al 2013), or the chemical evolution of Mn in the Galaxy (Seitenzahl et al 2013a), to distinguish between different explosion models.…”

Section: Introductionmentioning

confidence: 99%

5.9-keV Mn K-shell X-ray luminosity from the decay of 55Fe in Type Ia supernova models

Seitenzahl¹,

Krauß²,

Diehl³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We show that the X-ray line flux of the Mn K α line at 5.9 keV from the decay of 55 Fe is a promising diagnostic to distinguish between Type Ia supernova (SN Ia) explosion models. Using radiation transport calculations, we compute the line flux for two three-dimensional explosion models: a near-Chandrasekhar mass delayed detonation and a violent merger of two (1.1 and 0.9 M ⊙ ) white dwarfs. Both models are based on solar metallicity zero-age main sequence progenitors. Due to explosive nuclear burning at higher density, the delayeddetonation model synthesises ∼3.5 times more radioactive 55 Fe than the merger model. As a result, we find that the peak Mn K α line flux of the delayed-detonation model exceeds that of the merger model by a factor of ∼4.5. Since in both models the 5.9 keV X-ray flux peaks five to six years after the explosion, a single measurement of the X-ray line emission at this time can place a constraint on the explosion physics that is complementary to those derived from earlier phase optical spectra or light curves. We perform detector simulations of current and future X-ray telescopes to investigate the possibilities of detecting the X-ray line at 5.9 keV. Of the currently existing telescopes, XMM-Newton/pn is the best instrument for close ( 1 − 2 Mpc), non-background limited SNe Ia because of its large effective area. Due to its low instrumental background, Chandra/ACIS is currently the best choice for SNe Ia at distances above ∼2 Mpc. For the delayed-detonation scenario, a line detection is feasible with Chandra up to ∼3 Mpc for an exposure time of 10 6 s. We find that it should be possible with currently existing X-ray instruments (with exposure times 5 × 10 5 s) to detect both of our models at sufficiently high S/N to distinguish between them for hypothetical events within the Local Group. The prospects for detection will be better with future missions. For example, the proposed Athena/X-IFU instrument could detect our delayed-detonation model out to a distance of ∼5 Mpc. This would make it possible to study future events occurring during its operational life at distances comparable to those of the recent supernovae SN 2011fe (∼6.4 Mpc) and SN 2014J (∼3.5 Mpc).

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Detection of Circumstellar Material in a Normal Type Ia Supernova

Cited by 349 publications

References 21 publications

Constraining the progenitor of the Type Ia Supernova SN 2012cg

Constraining the progenitor of the Type Ia Supernova SN 2012cg

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

5.9-keV Mn K-shell X-ray luminosity from the decay of 55Fe in Type Ia supernova models

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